Both turbulence and magnetic fields are ubiquitous in astrophysical plasmas, and
they actively participate in diverse astrophysical processes, including the star formation,
cosmic ray propagation, and magnetic reconnection and particle acceleration in high-energy astrophysical environments
[1]}, [2]}, [3]}.
Turbulence is believed to be responsible for the amplification and maintenance of comic magnetic fields via the
“small-scale" turbulent dynamo mechanism
[4]}.
It refers to the amplification of magnetic fields due to the presence of turbulence
on scales below the driving scale of turbulence.
As the evidence for the magnetic field amplification via small-scale turbulent dynamo,
the measured magnetic energy spectra in diverse astrophysical media over a vast range of length scales
conform to the same spectral shape as the turbulent energy
(e.g., [5]}, [6]}, [7]}).
The dynamo amplification of magnetic fields and its implications have been studied
in diverse contexts, including the large-scale structure formation
[8]}, [9]}, [10]}, [11]},
(primordial) star formation and galaxy formation
[12]}, [13]}, [14]}, [15]}.
